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IceCube

IceCube. C. Spiering Saclay, Dec 2007. Congratulations to our ANTARES friends: 10 strings connected !. Content. Sources and signal expectations Neutrino telescopes under water and ice Physics results from AMANDA and Baikal IceCube: status, first results, prospects Summary. under-

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IceCube

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  1. IceCube C. Spiering Saclay, Dec 2007

  2. Congratulations to our ANTARES friends: 10 strings connected !

  3. Content • Sources and signal expectations • Neutrino telescopes under water and ice • Physics resultsfrom AMANDA and Baikal • IceCube: status, first results, prospects • Summary

  4. under- ground optical: - deep water - deep ice • air showers • radio • acoustics The unified spectrum of neutrinos

  5. Prominent Source Candidates Extra-Galactic Galactic AGN Galaxy Clusters GRB … SNR Microquasars Young SN shells …

  6. Prominent Source Candidates Extra-Galactic Galactic 1016-17 eV AGN Galaxy Clusters GRB … 1020-21 eV SNR Microquasars Young SN shells …

  7. Neutrino Production or e :  :  ~1:2:0 turns to 1:1:1 at Earth

  8.  bound MPR bound WB bound Diffuse Fluxes (1998) p + CMB p +

  9. Signal predictions: extragalactic sources • WB bound corresponds to 100-500 neutrinos per km²year • AGN predictions are highly uncertain (several orders of magnitude !) • Some of the older AGN models dramatically violate even soft upper bounds on diffuse fluxes, as derived from CR • Fluxes from individual AGN: less constrained • GRB: various models, benchmark model of Waxman-Bahcall can be easily tested with km3 detectors

  10. Signal predictions: galactic sources • Predictions on firmer ground than for AGN • Shell-type SNR • Pulsar Wind Nebula • Compact Binary Systems • Many papers in the last 2 years: • Bednarek and Montaruli 2005 • Vissani 2006 • DiStefano 2006 • Lipari 2006 • Kappes, Hinton, Stegmann, Aharonian 2007 • Gabici, Aharonian 2007 • … • Unanimous conclusion: Cubic kilometer detectors will just scrape the detection region

  11. Expected n flux from galactic point sources, example: RXJ 1713-3946 Assume p0 g and calculate related p±  n C. Stegmann ICRC 2007

  12. PKS2105-304 (R. White, ICRC) • PKS2105-304 as measured by H.E.S.S. • Correcting for  absorption • kinematics for / in source • KM3NeT with angular resolution 0.5° • S/Bg (> 1TeV) = 27/61 • S/Bg(> 5TeV) • =21/10 (5) R.J.White, ICRC

  13. muon tracks cascades Underwater/Ice: optical telescopes angle water < 0.3° water 3-6° (at 10 TeV) ice 0.5-1° ice ~25° (at 10 TeV) energy 0.3 in log E 30% in E (at 10 TeV)

  14. IceCube KM3NeT The Projects Baikal Antares Nestor, Nemo Amanda

  15. Baikal and AMANDA

  16. AMANDA-II ANTARES NT200 NT200+

  17. Basic parameters of present and planned neutrino telescopes Effective  area: • ~ 0.1 m² @ 10 TeV Amanda/Antares • ~ 4 m² @ 100 TeV Amanda/Antares • ~ 20 m² @ 100 TeV IceCube now • ~100 m² @ 100 TeV IceCube complete Point source sensitivity: • AMANDA, ANTARES:~ 310-10 / (cm² s) above 1 TeV • IceCube, KM3NeT ~ 10-11 / (cm² s) above 1 TeV (for 5 discovery)

  18. AMANDA Results

  19. Atmospheric neutrinos K. Münich RICAP 2007 spectrum measured up to 100 TeV

  20. 3 2 1 75o 60o 3 0 45o 2 -1 1 30o 0 -2 -1 15o -2 24h 0h -3 Search for steady point source AMANDA-II: 2000-2004 (1001 live days) 4282 n from Northern hemisphere No significant excess found

  21. Results for 2005

  22. 2005 data unbinned search 90% confidence level sensitivity to E-2 spectra

  23. Largest Excess: 3.6s d=48o , a=2.75h Log10(p-value) 69 out of 100 sky maps randomized in RA contain an excess of at least 3.6s 2005 Results

  24. ES 1959+650 WHIPPLE Flux of TeV photons (arb. units) Arrival time of neutrinos from the direction of the AGN ES1959+650 3   2 1 0 May June July 2000 2001 2002 2003 Year

  25. Diffuse fluxes • Atmospheric neutrinos behave like E-3.7 • Typical extraterrestrial fluxes behave like E-2

  26. Limit on diffuse extraterrestrial fluxes • Atmospheric neutrinos behave like E-3.7 • Typical extraterrestrial fluxes behave like E-2 • From this method and one year data we exclude E-2 fluxes with E2 > 2.710-7 GeV sr-1 s-1 cm-2

  27. Limit on diffuse extraterrestrial fluxes • From this method and one year data we exclude E-2 fluxes with E2 > 2.710-7 GeV sr-1 s-1 cm-2 • With 4 years and improved methods we are now at E2 > 8.810-8 GeV sr-1 s-1 cm-2

  28. Experimental limits & theoretical bounds • MPR bound, no neutron escape (gamma bound) • Factor 11 below MPR bound for sources opaque to neutrons

  29. Experimental limits & theoretical bounds • MPR bound, neutrons escape (CR bound) • Factor 4 below MPR bound for sources transparent to neutrons

  30. Experimental limits & theoretical bounds AGN core (SS) AGN Jet (MPR) GZK GRB (WB)

  31. Experimental limits & theoretical bounds old version AGN core (SS) „old“ Stecker model excluded

  32. Experimental limits & theoretical bounds AGN core (SS, new version) „new“ Stecker model not excluded (MRF = 1.9)

  33. Experimental limits & theoretical bounds AGN Jet (MPR) still above AGN jet (MPR) (MRF ~ 2.3) GRB (WB)

  34. Muon neutrinos Electron neutrinos Prompt Neutrinos from Charm Decay

  35. Limit on diffuse extraterrestrial fluxes AMANDA HE analysis Baikal IceCube muons, 1 year Icecube, muons & cascades 4 years 2003 2006 2009 2013 GRB (WB)

  36. Gamma Ray Bursts Vela Satellite 1969 Jet with G ~300-1000

  37. Coincidences with GRB Check for coincidences with BATSE, IPN, SWIFT 10-7 AMANDA limit from 408 bursts 1997-2003 10-8 • close to WB within < factor 2 • with IceCube: test WB within a few months Waxman-Bahcall GRB prediction E2flux (GeVcm-2s-1sr-1) 10-9 10-10 104 105 106 107 108 neutrino energy E(GeV)

  38. 107 monopole 105 d photons/cm 103 bare muon 101 0.4 0.6 0.8 1.0 b Relativistic Magnetic Monopoles Cherenkov Light  n2·(g/e)2 n = 1.33 (g/e) = 137/2  8300

  39. Relativistic Magnetic Monopoles Baikal 4 years AMANDA-II 1 year

  40. Relativistic Magnetic Monopoles IceCube-9 preliminary

  41. Earth Detector Neutralino Capture in the Sun Sun

  42. Sun Earth

  43. IceCube

  44. 2006-2007: 13 strings deployed 2005-2006: 8 strings 2004-2005 : 1 string 2007/08: add 14 to 18 strings and tank stations Completion by 2011. IceCube IceTop Current configuration - 22 strings - 52 surface tanks Air shower detector 80 pairs of ice Cherenkov tanks Threshold ~ 300 TeV 1450m InIce AMANDA-II 19 strings 677 modules Goal of 80 strings of 60 optical modules each 17 m between modules 125 m string separation AMANDA now operating as part of IceCube AMANDA now operating as part of IceCube 2450m

  45. IceCube IceTop Current configuration - 22 strings - 52 surface tanks Air shower detector 80 pairs of ice Cherenkov tanks Threshold ~ 300 TeV • IceTop • Angular calibration • of IceCube • chemical composition • (with IceCube) • veto for IceCube 1450m InIce Goal of 80 strings of 60 optical modules each 17 m between modules 125 m string separation 2450m

  46. IceCube 2006-2007: 13 strings deployed IceTop Current configuration - 22 strings - 52 surface tanks Air shower detector 80 pairs of ice Cherenkov tanks Threshold ~ 300 TeV 2005-2006: 8 strings 1450m InIce AMANDA-II 19 strings 677 modules Goal of 80 strings of 60 optical modules each 17 m between modules 125 m string separation AMANDA now operating as part of IceCube AMANDA now operating as part of IceCube 2450m

  47. Measured Effective Scattering Coefficient IceCube Coll, J. Geophys. Res. 111 (2006) D13203

  48. IceCube

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